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Astrometry and Photometry of Trapezium–Type Multiple Stars1

Published online by Cambridge University Press:  12 April 2016

P.L. Bernacca ,
M.G. Lattanzi  and
G. Massone
P.L. Bernacca
Affiliation:
Asiago Astrophysical Observatory, Italy
M.G. Lattanzi
Affiliation:
Torino Astronomical Observatory, Italy ESA, Space Science Division, at STScI, USA
G. Massone
Affiliation:
Torino Astronomical Observatory, Italy

Extract

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Trapezia systems are defined as multiple stars, having three or more components with separation ratios in the range 0.3 to 3. The revival of interest in Trapezia is due to their potential astrophysical significance, as they could originate from a single protostar and be in an expansion stage because of their possible positive energy (see, for example, Bernacca 1988 and references therein). Further decisive advancements in understanding the nature of these systems require data for establishing a list of physically bound systems as well as for the systematic study of their kinematics and energetics. In the present progress report we test three representative cases with the combined exploitation of astrometric, photometric, and spectroscopic data.

Type
Classical Methods, Catalogs, & Databases
Information
International Astronomical Union Colloquium , Volume 135: Complementary Approaches to Double and Multiple Star Research , 1992 , pp. 303 - 307
Copyright
Copyright © Astronomical Society of the Pacific 1992

Footnotes

1

Based in put on observations taken at the Europen Southern Observatory (La Silla, Chile) on Dec 1988

References

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